Non-linear model of particle acceleration at colliding shock flows

被引：35

作者：

Bykov, A. M. ^{[1
,2
]}

Gladilin, P. E. ^{[1
,2
]}

Osipov, S. M. ^{[1
,2
]}

机构：

[1] Russian Acad Sci, AF Ioffe Phys Tech Inst, St Petersburg 196140, Russia

[2] St Petersburg State Polytech Univ, St Petersburg, Russia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 429卷 / 03期

关键词：

acceleration of particles; shock waves; GAMMA-RAY EMISSION; COSMIC-RAYS; MAGNETIC-FIELD; X-RAY; SUPERNOVA-REMNANTS; SPECTRUM; RADIO; TURBULENCE;

D O I：

10.1093/mnras/sts553

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Powerful stellar winds and supernova explosions with intense energy release in the form of strong shock waves can convert a sizeable part of the kinetic energy release into energetic particles. The star-forming regions are argued as a favourable site of energetic particle acceleration and could be efficient sources of non-thermal emission. We present here a non-linear time-dependent model of particle acceleration in the vicinity of two closely approaching fast magnetohydrodynamic (MHD) shocks. Such MHD flows are expected to occur in rich young stellar cluster where a supernova is exploding in the vicinity of a strong stellar wind of a nearby massive star. We find that the spectrum of the high-energy particles accelerated at the stage of two closely approaching shocks can be harder than that formed at a forward shock of an isolated supernova remnant. The presented method can be applied to model particle acceleration in a variety of systems with colliding MHD flows.

引用

页码：2755 / 2762

页数：8

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